Nova Ejecta Abundances Resulting from Multi-Cycle Evolutionary Calculations

  • Dina Prialnik
  • Attay Kovetz
Part of the Astrophysics and Space Science Library book series (ASSL, volume 208)

Abstract

The theory of nova outbursts invokes accretion of hydrogen-rich material by a white dwarf (WD) in a close binary system, due to Roche lobe overflow of a red dwarf companion, leading to periodic outbursts — powered by thermonuclear runaways — that result in mass ejection. Observed characteristics of novae are reproduced by varying the values of three basic and independent parameters: the accreting white dwarf’s mass, its core temperature, and the mass transfer rate. In a recent study (Prialnik & Kovetz 1995) we have carried out a systematic investigation of nova outbursts on WD progenitors composed of C and O in equal mass fractions, concluding that the entire range of observed nova characteristics could be accounted for. A subset of 34 out of 64 evolutionary sequences (obtained with different parameter combinations) reproduced classical novae, and here we focus on the break-up of the heavy element abundances in the ejecta of these models, in comparison with observations, based on a recent analysis of observed nova abundances by Livio & Truran (1994).

Keywords

Mass Transfer Rate White Dwarf Close Binary System Cataclysmic Variable Heavy Element Abundance 
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References

  1. Iben, I. Jr., Tutukov, A.V., 1985, Ap. J. Supp., 58, 661ADSCrossRefGoogle Scholar
  2. Livio, M., Truran, J.W., 1994, Ap. J., 425, 797ADSCrossRefGoogle Scholar
  3. Prialnik, D., Kovetz, A., 1995, Ap. J., 445, 789ADSCrossRefGoogle Scholar

Copyright information

© Kluwer Academic Publishers 1996

Authors and Affiliations

  • Dina Prialnik
    • 1
  • Attay Kovetz
    • 2
  1. 1.Department of Geophysics and Planetary SciencesUSA
  2. 2.School of Physics and Astronomy Tel Aviv UniversityRamat AvivIsrael

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